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Recent ALMA observations have unveiled a wealth of fine structures in star-forming regions, such as protostellar outflows and jets, asymmetric gas accretion, and rotationally supported circumstellar disks. In addition, ring and gap substructures—often interpreted as signatures of planet formation—have been identified even during the active gas accretion phase. In this study, we carried out magnetohydrodynamic simulations of star formation starting from a prestellar core, and followed the subsequent formation and evolution of a protostar and its surrounding disk up to the Class II stage. Our simulations successfully reproduce the development of outflows and jets, as well as circumstellar disks exhibiting complex morphologies, envelopes, and asymmetric accretion flows. By comparing these results with ALMA observations, we gain insight into the physical processes governing the earliest stages of star and disk formation. In this talk, I will present recent progress in our understanding of early star formation based on comparisons between numerical simulations and observations.